The GOGREEN Survey: A deep stellar mass function of cluster galaxies at 1.0 < z < 1.4 and the complex nature of satellite quenching
We study the stellar mass functions (SMFs) of star-forming and quiescent galaxies in 11 galaxy clusters at 1.0
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| Veröffentlicht in: | Astronomy and astrophysics (Berlin) 2020-06, Vol.638, p.A112 |
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| creator | van der Burg, Remco F. J. Rudnick, Gregory Balogh, Michael L. Muzzin, Adam Lidman, Chris Old, Lyndsay J. Shipley, Heath Gilbank, David McGee, Sean Biviano, Andrea Cerulo, Pierluigi Chan, Jeffrey C. C. Cooper, Michael De Lucia, Gabriella Demarco, Ricardo Forrest, Ben Gwyn, Stephen Jablonka, Pascale Kukstas, Egidijus Marchesini, Danilo Nantais, Julie Noble, Allison Pintos-Castro, Irene Poggianti, Bianca Reeves, Andrew M. M. Stefanon, Mauro Vulcani, Benedetta Webb, Kristi Wilson, Gillian Yee, Howard Zaritsky, Dennis |
| description | We study the stellar mass functions (SMFs) of star-forming and quiescent galaxies in 11 galaxy clusters at 1.0 |
| doi_str_mv | 10.1051/0004-6361/202037754 |
| format | Article |
| fullrecord | <record><control><sourceid>proquest_hal_p</sourceid><recordid>TN_cdi_hal_primary_oai_HAL_hal_03224230v1</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>2487122516</sourcerecordid><originalsourceid>FETCH-LOGICAL-c422t-df45d642ac3b91f3ff4437ac2edbc626f985d5ba03dd3b56ffd331fedfe7b9b03</originalsourceid><addsrcrecordid>eNo9kc1OwkAQxzdGExF9Ai-TePJQ2K-2YLwQgmBCJFE8b7b7ASWlxd2WgG_gW_AsPJmtGE6Tmfnll8l_ELonuENwSLoYYx5ELCJdiilmcRzyC9QinNEAxzy6RK0zcY1uvF_VLSU91kI_86WB8Wz8Phq9wUfltmb_BAPQxmzAlybLpIO19B5slasyLXIoLKisqncOFjKTu9R4kCWQDj4eno8H-Ia_SjocZK6hrP2qWG8ys4NclpUzjcHLxp2WBr4qk6tlmi9u0ZWVmTd3_7WNPl9G8-EkmM7Gr8PBNFCc0jLQloc64lQqlvSJZdZyzmKpqNGJimhk-71Qh4nETGuWhJG1mjFijbYmTvoJZm30ePIuZSY2Ll1LtxeFTMVkMBXNDDNKOWV4S2r24cRuXFEf6kuxKiqX1-cJynsxoTQkUU2xE6Vc4b0z9qwlWDT_EU36oklfnP_DfgGrVIRf</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>2487122516</pqid></control><display><type>article</type><title>The GOGREEN Survey: A deep stellar mass function of cluster galaxies at 1.0 < z < 1.4 and the complex nature of satellite quenching</title><source>Bacon EDP Sciences France Licence nationale-ISTEX-PS-Journals-PFISTEX</source><source>EDP Sciences</source><source>Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals</source><creator>van der Burg, Remco F. J. ; Rudnick, Gregory ; Balogh, Michael L. ; Muzzin, Adam ; Lidman, Chris ; Old, Lyndsay J. ; Shipley, Heath ; Gilbank, David ; McGee, Sean ; Biviano, Andrea ; Cerulo, Pierluigi ; Chan, Jeffrey C. C. ; Cooper, Michael ; De Lucia, Gabriella ; Demarco, Ricardo ; Forrest, Ben ; Gwyn, Stephen ; Jablonka, Pascale ; Kukstas, Egidijus ; Marchesini, Danilo ; Nantais, Julie ; Noble, Allison ; Pintos-Castro, Irene ; Poggianti, Bianca ; Reeves, Andrew M. M. ; Stefanon, Mauro ; Vulcani, Benedetta ; Webb, Kristi ; Wilson, Gillian ; Yee, Howard ; Zaritsky, Dennis</creator><creatorcontrib>van der Burg, Remco F. J. ; Rudnick, Gregory ; Balogh, Michael L. ; Muzzin, Adam ; Lidman, Chris ; Old, Lyndsay J. ; Shipley, Heath ; Gilbank, David ; McGee, Sean ; Biviano, Andrea ; Cerulo, Pierluigi ; Chan, Jeffrey C. C. ; Cooper, Michael ; De Lucia, Gabriella ; Demarco, Ricardo ; Forrest, Ben ; Gwyn, Stephen ; Jablonka, Pascale ; Kukstas, Egidijus ; Marchesini, Danilo ; Nantais, Julie ; Noble, Allison ; Pintos-Castro, Irene ; Poggianti, Bianca ; Reeves, Andrew M. M. ; Stefanon, Mauro ; Vulcani, Benedetta ; Webb, Kristi ; Wilson, Gillian ; Yee, Howard ; Zaritsky, Dennis</creatorcontrib><description>We study the stellar mass functions (SMFs) of star-forming and quiescent galaxies in 11 galaxy clusters at 1.0 <
z
< 1.4 drawn from the Gemini Observations of Galaxies in Rich Early ENvironments (GOGREEN) survey. Based on more than 500 h of Gemini/GMOS spectroscopy and deep multi-band photometry taken with a range of observatories, we probe the SMFs down to a stellar mass limit of 10
9.7
M
⊙
(10
9.5
M
⊙
for star-forming galaxies). At this early epoch, the fraction of quiescent galaxies is already highly elevated in the clusters compared to the field at the same redshift. The quenched fraction excess (QFE) represents the fraction of galaxies that would be star-forming in the field but are quenched due to their environment. The QFE is strongly mass dependent, and increases from ∼30% at
M
⋆
= 10
9.7
M
⊙
to ∼80% at
M
⋆
= 10
11.0
M
⊙
. Nonetheless, the shapes of the SMFs of the two individual galaxy types, star-forming and quiescent galaxies, are identical between cluster and field to high statistical precision. Nevertheless, along with the different quiescent fractions, the total galaxy SMF is also environmentally dependent, with a relative deficit of low-mass galaxies in the clusters. These results are in stark contrast with findings in the local Universe, and therefore require a substantially different quenching mode to operate at early times. We discuss these results in light of several popular quenching models.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0746</identifier><identifier>EISSN: 1432-0756</identifier><identifier>DOI: 10.1051/0004-6361/202037754</identifier><language>eng</language><publisher>Heidelberg: EDP Sciences</publisher><subject>Astrophysics ; Galaxies ; Observatories ; Physics ; Quenching ; Red shift ; Star formation ; Stars & galaxies ; Stellar mass</subject><ispartof>Astronomy and astrophysics (Berlin), 2020-06, Vol.638, p.A112</ispartof><rights>Copyright EDP Sciences Jun 2020</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c422t-df45d642ac3b91f3ff4437ac2edbc626f985d5ba03dd3b56ffd331fedfe7b9b03</citedby><cites>FETCH-LOGICAL-c422t-df45d642ac3b91f3ff4437ac2edbc626f985d5ba03dd3b56ffd331fedfe7b9b03</cites><orcidid>0000-0003-1535-2327 ; 0000-0003-3921-2177 ; 0000-0001-8221-8406 ; 0000-0003-1731-0497 ; 0000-0002-5177-727X ; 0000-0001-5851-1856 ; 0000-0002-6220-9104 ; 0000-0001-6251-3125 ; 0000-0002-9655-1063 ; 0000-0001-7768-5309 ; 0000-0002-8610-0672 ; 0000-0002-7356-0629 ; 0000-0003-2618-6408 ; 0000-0003-0980-1499 ; 0000-0003-3255-3139</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,314,776,780,881,3714,27901,27902</link.rule.ids><backlink>$$Uhttps://hal.science/hal-03224230$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>van der Burg, Remco F. J.</creatorcontrib><creatorcontrib>Rudnick, Gregory</creatorcontrib><creatorcontrib>Balogh, Michael L.</creatorcontrib><creatorcontrib>Muzzin, Adam</creatorcontrib><creatorcontrib>Lidman, Chris</creatorcontrib><creatorcontrib>Old, Lyndsay J.</creatorcontrib><creatorcontrib>Shipley, Heath</creatorcontrib><creatorcontrib>Gilbank, David</creatorcontrib><creatorcontrib>McGee, Sean</creatorcontrib><creatorcontrib>Biviano, Andrea</creatorcontrib><creatorcontrib>Cerulo, Pierluigi</creatorcontrib><creatorcontrib>Chan, Jeffrey C. C.</creatorcontrib><creatorcontrib>Cooper, Michael</creatorcontrib><creatorcontrib>De Lucia, Gabriella</creatorcontrib><creatorcontrib>Demarco, Ricardo</creatorcontrib><creatorcontrib>Forrest, Ben</creatorcontrib><creatorcontrib>Gwyn, Stephen</creatorcontrib><creatorcontrib>Jablonka, Pascale</creatorcontrib><creatorcontrib>Kukstas, Egidijus</creatorcontrib><creatorcontrib>Marchesini, Danilo</creatorcontrib><creatorcontrib>Nantais, Julie</creatorcontrib><creatorcontrib>Noble, Allison</creatorcontrib><creatorcontrib>Pintos-Castro, Irene</creatorcontrib><creatorcontrib>Poggianti, Bianca</creatorcontrib><creatorcontrib>Reeves, Andrew M. M.</creatorcontrib><creatorcontrib>Stefanon, Mauro</creatorcontrib><creatorcontrib>Vulcani, Benedetta</creatorcontrib><creatorcontrib>Webb, Kristi</creatorcontrib><creatorcontrib>Wilson, Gillian</creatorcontrib><creatorcontrib>Yee, Howard</creatorcontrib><creatorcontrib>Zaritsky, Dennis</creatorcontrib><title>The GOGREEN Survey: A deep stellar mass function of cluster galaxies at 1.0 < z < 1.4 and the complex nature of satellite quenching</title><title>Astronomy and astrophysics (Berlin)</title><description>We study the stellar mass functions (SMFs) of star-forming and quiescent galaxies in 11 galaxy clusters at 1.0 <
z
< 1.4 drawn from the Gemini Observations of Galaxies in Rich Early ENvironments (GOGREEN) survey. Based on more than 500 h of Gemini/GMOS spectroscopy and deep multi-band photometry taken with a range of observatories, we probe the SMFs down to a stellar mass limit of 10
9.7
M
⊙
(10
9.5
M
⊙
for star-forming galaxies). At this early epoch, the fraction of quiescent galaxies is already highly elevated in the clusters compared to the field at the same redshift. The quenched fraction excess (QFE) represents the fraction of galaxies that would be star-forming in the field but are quenched due to their environment. The QFE is strongly mass dependent, and increases from ∼30% at
M
⋆
= 10
9.7
M
⊙
to ∼80% at
M
⋆
= 10
11.0
M
⊙
. Nonetheless, the shapes of the SMFs of the two individual galaxy types, star-forming and quiescent galaxies, are identical between cluster and field to high statistical precision. Nevertheless, along with the different quiescent fractions, the total galaxy SMF is also environmentally dependent, with a relative deficit of low-mass galaxies in the clusters. These results are in stark contrast with findings in the local Universe, and therefore require a substantially different quenching mode to operate at early times. We discuss these results in light of several popular quenching models.</description><subject>Astrophysics</subject><subject>Galaxies</subject><subject>Observatories</subject><subject>Physics</subject><subject>Quenching</subject><subject>Red shift</subject><subject>Star formation</subject><subject>Stars & galaxies</subject><subject>Stellar mass</subject><issn>0004-6361</issn><issn>1432-0746</issn><issn>1432-0756</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2020</creationdate><recordtype>article</recordtype><recordid>eNo9kc1OwkAQxzdGExF9Ai-TePJQ2K-2YLwQgmBCJFE8b7b7ASWlxd2WgG_gW_AsPJmtGE6Tmfnll8l_ELonuENwSLoYYx5ELCJdiilmcRzyC9QinNEAxzy6RK0zcY1uvF_VLSU91kI_86WB8Wz8Phq9wUfltmb_BAPQxmzAlybLpIO19B5slasyLXIoLKisqncOFjKTu9R4kCWQDj4eno8H-Ia_SjocZK6hrP2qWG8ys4NclpUzjcHLxp2WBr4qk6tlmi9u0ZWVmTd3_7WNPl9G8-EkmM7Gr8PBNFCc0jLQloc64lQqlvSJZdZyzmKpqNGJimhk-71Qh4nETGuWhJG1mjFijbYmTvoJZm30ePIuZSY2Ll1LtxeFTMVkMBXNDDNKOWV4S2r24cRuXFEf6kuxKiqX1-cJynsxoTQkUU2xE6Vc4b0z9qwlWDT_EU36oklfnP_DfgGrVIRf</recordid><startdate>20200601</startdate><enddate>20200601</enddate><creator>van der Burg, Remco F. 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M.</creator><creator>Stefanon, Mauro</creator><creator>Vulcani, Benedetta</creator><creator>Webb, Kristi</creator><creator>Wilson, Gillian</creator><creator>Yee, Howard</creator><creator>Zaritsky, Dennis</creator><general>EDP Sciences</general><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>1XC</scope><scope>VOOES</scope><orcidid>https://orcid.org/0000-0003-1535-2327</orcidid><orcidid>https://orcid.org/0000-0003-3921-2177</orcidid><orcidid>https://orcid.org/0000-0001-8221-8406</orcidid><orcidid>https://orcid.org/0000-0003-1731-0497</orcidid><orcidid>https://orcid.org/0000-0002-5177-727X</orcidid><orcidid>https://orcid.org/0000-0001-5851-1856</orcidid><orcidid>https://orcid.org/0000-0002-6220-9104</orcidid><orcidid>https://orcid.org/0000-0001-6251-3125</orcidid><orcidid>https://orcid.org/0000-0002-9655-1063</orcidid><orcidid>https://orcid.org/0000-0001-7768-5309</orcidid><orcidid>https://orcid.org/0000-0002-8610-0672</orcidid><orcidid>https://orcid.org/0000-0002-7356-0629</orcidid><orcidid>https://orcid.org/0000-0003-2618-6408</orcidid><orcidid>https://orcid.org/0000-0003-0980-1499</orcidid><orcidid>https://orcid.org/0000-0003-3255-3139</orcidid></search><sort><creationdate>20200601</creationdate><title>The GOGREEN Survey: A deep stellar mass function of cluster galaxies at 1.0 < z < 1.4 and the complex nature of satellite quenching</title><author>van der Burg, Remco F. J. ; Rudnick, Gregory ; Balogh, Michael L. ; Muzzin, Adam ; Lidman, Chris ; Old, Lyndsay J. ; Shipley, Heath ; Gilbank, David ; McGee, Sean ; Biviano, Andrea ; Cerulo, Pierluigi ; Chan, Jeffrey C. C. ; Cooper, Michael ; De Lucia, Gabriella ; Demarco, Ricardo ; Forrest, Ben ; Gwyn, Stephen ; Jablonka, Pascale ; Kukstas, Egidijus ; Marchesini, Danilo ; Nantais, Julie ; Noble, Allison ; Pintos-Castro, Irene ; Poggianti, Bianca ; Reeves, Andrew M. 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M.</creatorcontrib><creatorcontrib>Stefanon, Mauro</creatorcontrib><creatorcontrib>Vulcani, Benedetta</creatorcontrib><creatorcontrib>Webb, Kristi</creatorcontrib><creatorcontrib>Wilson, Gillian</creatorcontrib><creatorcontrib>Yee, Howard</creatorcontrib><creatorcontrib>Zaritsky, Dennis</creatorcontrib><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Hyper Article en Ligne (HAL)</collection><collection>Hyper Article en Ligne (HAL) (Open Access)</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>van der Burg, Remco F. J.</au><au>Rudnick, Gregory</au><au>Balogh, Michael L.</au><au>Muzzin, Adam</au><au>Lidman, Chris</au><au>Old, Lyndsay J.</au><au>Shipley, Heath</au><au>Gilbank, David</au><au>McGee, Sean</au><au>Biviano, Andrea</au><au>Cerulo, Pierluigi</au><au>Chan, Jeffrey C. C.</au><au>Cooper, Michael</au><au>De Lucia, Gabriella</au><au>Demarco, Ricardo</au><au>Forrest, Ben</au><au>Gwyn, Stephen</au><au>Jablonka, Pascale</au><au>Kukstas, Egidijus</au><au>Marchesini, Danilo</au><au>Nantais, Julie</au><au>Noble, Allison</au><au>Pintos-Castro, Irene</au><au>Poggianti, Bianca</au><au>Reeves, Andrew M. M.</au><au>Stefanon, Mauro</au><au>Vulcani, Benedetta</au><au>Webb, Kristi</au><au>Wilson, Gillian</au><au>Yee, Howard</au><au>Zaritsky, Dennis</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The GOGREEN Survey: A deep stellar mass function of cluster galaxies at 1.0 < z < 1.4 and the complex nature of satellite quenching</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2020-06-01</date><risdate>2020</risdate><volume>638</volume><spage>A112</spage><pages>A112-</pages><issn>0004-6361</issn><eissn>1432-0746</eissn><eissn>1432-0756</eissn><abstract>We study the stellar mass functions (SMFs) of star-forming and quiescent galaxies in 11 galaxy clusters at 1.0 <
z
< 1.4 drawn from the Gemini Observations of Galaxies in Rich Early ENvironments (GOGREEN) survey. Based on more than 500 h of Gemini/GMOS spectroscopy and deep multi-band photometry taken with a range of observatories, we probe the SMFs down to a stellar mass limit of 10
9.7
M
⊙
(10
9.5
M
⊙
for star-forming galaxies). At this early epoch, the fraction of quiescent galaxies is already highly elevated in the clusters compared to the field at the same redshift. The quenched fraction excess (QFE) represents the fraction of galaxies that would be star-forming in the field but are quenched due to their environment. The QFE is strongly mass dependent, and increases from ∼30% at
M
⋆
= 10
9.7
M
⊙
to ∼80% at
M
⋆
= 10
11.0
M
⊙
. Nonetheless, the shapes of the SMFs of the two individual galaxy types, star-forming and quiescent galaxies, are identical between cluster and field to high statistical precision. Nevertheless, along with the different quiescent fractions, the total galaxy SMF is also environmentally dependent, with a relative deficit of low-mass galaxies in the clusters. These results are in stark contrast with findings in the local Universe, and therefore require a substantially different quenching mode to operate at early times. We discuss these results in light of several popular quenching models.</abstract><cop>Heidelberg</cop><pub>EDP Sciences</pub><doi>10.1051/0004-6361/202037754</doi><orcidid>https://orcid.org/0000-0003-1535-2327</orcidid><orcidid>https://orcid.org/0000-0003-3921-2177</orcidid><orcidid>https://orcid.org/0000-0001-8221-8406</orcidid><orcidid>https://orcid.org/0000-0003-1731-0497</orcidid><orcidid>https://orcid.org/0000-0002-5177-727X</orcidid><orcidid>https://orcid.org/0000-0001-5851-1856</orcidid><orcidid>https://orcid.org/0000-0002-6220-9104</orcidid><orcidid>https://orcid.org/0000-0001-6251-3125</orcidid><orcidid>https://orcid.org/0000-0002-9655-1063</orcidid><orcidid>https://orcid.org/0000-0001-7768-5309</orcidid><orcidid>https://orcid.org/0000-0002-8610-0672</orcidid><orcidid>https://orcid.org/0000-0002-7356-0629</orcidid><orcidid>https://orcid.org/0000-0003-2618-6408</orcidid><orcidid>https://orcid.org/0000-0003-0980-1499</orcidid><orcidid>https://orcid.org/0000-0003-3255-3139</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
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| ispartof | Astronomy and astrophysics (Berlin), 2020-06, Vol.638, p.A112 |
| issn | 0004-6361 1432-0746 1432-0756 |
| language | eng |
| recordid | cdi_hal_primary_oai_HAL_hal_03224230v1 |
| source | Bacon EDP Sciences France Licence nationale-ISTEX-PS-Journals-PFISTEX; EDP Sciences; Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals |
| subjects | Astrophysics Galaxies Observatories Physics Quenching Red shift Star formation Stars & galaxies Stellar mass |
| title | The GOGREEN Survey: A deep stellar mass function of cluster galaxies at 1.0 < z < 1.4 and the complex nature of satellite quenching |
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